Three-Dimensional Interaction between a Planet and an Isothermal Gaseous Disk. I. Corotation and Lindblad Torques and Planet Migration

By Hidekazu Tanaka, T. Takeuchi, W. Ward. 2002

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In Astronomy and Astrophysics

Citations in the corpus

WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, result): “On the contrary, they argued that this result is inconsistent with a disk-driven migration scenario (e.g. Goldreich & Tremaine 1980, Lin & Papaloizou 1986, Tanaka et al. 2002, Lubow & Ida 2010), as the inner edge of the orbital period distribution should then be right at the Roche limit.”
Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants (2018, neutral): “The migration timescale τmig of lowmass planets is estimated in Tanaka et al. (2002) and given as τmig = C M Mpl M Σg(rpl)r2pl (H r )2 pl Ω−1K ≈ 7.8 × 105 ( Mpl ME )−1 yr .”
THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “Disk migration At low masses, planets within a gaseous disk undergo type I disk migration (Tanaka et al. 2002).”
Halting type I planet migration in non-isothermal disks (2006, background): “The disk response is linear in this case, and the resulting torques can be calculated in a semi-analytic way (Tanaka et al. 2002).”
BINARY BLACK HOLE ACCRETION FROM A CIRCUMBINARY DISK: GAS DYNAMICS INSIDE THE CENTRAL CAVITY (2013, methodology): “(13) Here, we have followed Duffell & MacFadyen (2013); Tanaka et al. (2002); Masset (2002); Müller et al. (2012) and used a “vertically averaged” potential which attempts to account for corrections to the gravitational force near each point mass due to the nonzero thickness of the disk.”
Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, methodology): “This means that it migrates on a viscous timescale, which is typically much longer than the migration timescale in the isothermal type I approximation (Tanaka et al. 2002).”
PLANETARY POPULATION SYNTHESIS COUPLED WITH ATMOSPHERIC ESCAPE: A STATISTICAL VIEW OF EVAPORATION (2014, methodology): “Synthetic Planets: C, non-isothermal Migration and Different Grain Opacities Various evaporation models have been applied to the nominal planet population that is calculated using the isothermal type I migration rate reduced by a factor of 0.1 Tanaka et al. (2002).”
The effect of gas drag on the growth of protoplanets. Analytical expressions for the accretion of small bodies in laminar disks (2010, background): “Likewise, type-I radial migration (Tanaka et al. 2002) is not incorporated in our framework.”
Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “For example, the efficiency of type I migration needed to be reduced considerably (10 to a 1000 times) from the linear rate by Tanaka et al. (2002) otherwise it would have been impossible to reproduce the observed semimajor axis distribution (but see also Ida & Lin 2008b).”
Migration and the Formation of Systems of Hot Super-Earths and Neptunes (2006, background): “In the local treatment of type I migration (e.g., Tanaka et al. 2002), if the planet is not in contact with the disk, there is no interaction between them so that tm,i, t d e,i and ti,i are taken to be infinite.”
A torque formula for non-isothermal type I planetary migration – I. Unsaturated horseshoe drag (2009, methodology): “This yields a Lindblad torque (Tanaka et al. 2002, their 2D result): L/ 0 = −3.2 − 1.468α, (7) with2 0 = (q/h)2 pr4p 2p (8) and a corotation torque c,lin/ 0 = 2.04 − 1.36α. (9) Note that the linear corotation torque is proportional to the radial gradient of specific vorticity (Goldreich & Tremaine…”
IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, background): “The origins of the Super-Earth population are widely debated, and both migration-based models (Terquem and Papaloizou 2007; Cresswell and Nelson 2008) as well as in situ accretion scenarios (Hansen and Murray 2012; Chiang and Laughlin 2013) have been proposed to explain the data.”
The Evolution of Gravitationally Unstable Protoplanetary Disks: Fragmentation and Possible Giant Planet Formation (2003, background): “As a consequence (Ward 1997a, 1997b; Tanaka et al. 2002), we do not expect migration to occur on the viscous timescale of the disk as in the classic type II regime, and indeed, no clear gap is visible.”
Toward a Deterministic Model of Planetary Formation. IV. Effects of Type I Migration (2008, methodology): “From the linear analysis, the characteristic orbital decay timescale of Earth-mass cores at several AUs in a MMSN model is about 1 Myr (Ward 1986; Tanaka et al. 2002).”
Planet Formation around Stars of Various Masses: The Snow Line and the Frequency of Giant Planets (2007, methodology): “We have chosen to ignore type I migration, where linear theory predicts that protoplanets excite spiral density waves in the gas disk, and migrate toward the central star on 0.01–0.1Myr timescales (Tanaka et al. 2002).”